Setting the stage for the Solar System formation

Meteorites display an isotopic composition dichotomy between non-carbonaceous (NC) and carbonaceous (CC) groups, indicating that planetesimal formation in the solar protoplanetary disk occurred in two distinct reservoirs. A new model will be introduced to explain this dichotomy from the circumstance that the arrival of the outer CC dust particles in the inner disk is delayed for several million years by the viscous expansion of the protoplanetary disk.
Besides, hydrodynamical modeling has shown that while the Sun's gaseous protoplanetary disk was present, the giant planets migrated into a compact orbital configuration in a chain of resonances. I will show that the giant planets's dynamical instability was likely triggered by the inside-out dispersal of the gaseous disk. Such an instability took place as the disk dissipated, constrained to be a few to ten million years after the birth of the Solar System.

Beibei LIU (ZJU)
Join Zoom Meeting Meeting ID: 864 5332 2468 Passcode: 258990
Ke Wang
Thursday, November 10, 2022 - 3:30PM to Thursday, November 10, 2022 - 4:30PM
Prof Liu obtained PhD from Peking University in 2015, and then moved to University of Amsterdam and Lund University as postdocs. In 2020 he joined Zhejiang University. Research interest: the formation and dynamical evolution of the solar system and exoplanets.